Mathematics – Logic
Scientific paper
Dec 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufm.p23a1703c&link_type=abstract
American Geophysical Union, Fall Meeting 2011, abstract #P23A-1703
Mathematics
Logic
[6017] Planetary Sciences: Comets And Small Bodies / Erosion And Weathering, [6225] Planetary Sciences: Solar System Objects / Mars
Scientific paper
Moreux crater is a 135 km-diameter impact basin situated at 42.1° north latitude and 315.6° west longitude. Its location, just north of Arabia Terra, is situated at the edge of a plateau of southern highlands, and its southern portion represents the dichotomy boundary, dislocating the regional scarp[1]. Morphologic features inside the crater suggest that its interior has been shaped by the action of diverse processes[2]. Recently, aeolian features have also been reported[3],[4]. A GIS was utilized to gather data from different Mars mission instruments. HiRISE and CTX data from MRO mission were use to analyze the geomorphologic pattern of the dunes whereas the CRISM for Mars observations brought information relative to their mineralogy. CRISM data were processed and analyzed as described in Murchie et al. [2009] [5]. We observed Large Dark Dunes (LDD) all around the crater central peak. Ergs consist of a mix of barchans, barchanoids, transverse dunes but also star dunes, domes and linear dunes are present. We also identified bright bedforms, the TARs. Our morphological analysis suggests that the aforementioned aeolian features developed under a multi-directional wind regime. The dune morphology even suggests diverse episodes of aeolian deposition sustained by changes in wind direction[4].CRISM spectra extracted from the LDD show that these dunes are bearing strong mafic signatures. Spectra from the LDD generally have a strong and broad 1.250 μm absorption band, which is consistent with olivine. This large band is actually a combination of 3 absorptions centered at 850, 1050 and 1250 nm[6].The shape of the spectra is especially consistent with fayalite, or large grain olivine-rich sands [7].On a few observations, an additional wide band around 2.1 μm is present in the spectra. This band characterizes the presence of high-calcium pyroxene, which seems to be the dominant mineral of the dune-free areas. Contrary to pyroxenes, olivine minerals seem to occur solely in the dunes and not in the surrounding thin windblown sand sheets. Due to their spatial resolution, limited to 18 m/pixel at maximum, CRISM data could not be used to characterize the TAR composition. These preliminary results are consistent with the composition of most martian dark dunes [8]. Further analyses are to be done and should help determining the potential source for the dune sediments, and whether this source is local [8].
Cardinale Marco
Flahaut Jessica
Komatsu Goro
No associations
LandOfFree
Large dark dunes in Moreux Crater, Mars: Insights into their geometry and composition. M. Cardinale1, J. Flahaut2, G. Komatsu1, (1) International Research School of Planetary Sciences, Università D'Annunzio, Viale Pindaro 42, 65127 Pescara, Italy. (2) Labo does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Large dark dunes in Moreux Crater, Mars: Insights into their geometry and composition. M. Cardinale1, J. Flahaut2, G. Komatsu1, (1) International Research School of Planetary Sciences, Università D'Annunzio, Viale Pindaro 42, 65127 Pescara, Italy. (2) Labo, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Large dark dunes in Moreux Crater, Mars: Insights into their geometry and composition. M. Cardinale1, J. Flahaut2, G. Komatsu1, (1) International Research School of Planetary Sciences, Università D'Annunzio, Viale Pindaro 42, 65127 Pescara, Italy. (2) Labo will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-869635